A reappraisal of the habitability of planets around M dwarf stars

Stable, hydrogen-burning, M dwarf stars make up about 75% of all stars in the Galaxy. They are extremely long-lived, and because they are much smaller in mass than the Sun (between 0.5 and 0.08 M(Sun)), their temperature and stellar luminosity are low and peaked in the red. We have re-examined what is known at present about the potential for a terrestrial planet forming within, or migrating into, the classic liquid-surface-water habitable zone close to an M dwarf star. Observations of protoplanetary disks suggest that planet-building materials are common around M dwarfs, but N-body simulations differ in their estimations of the likelihood of potentially habitable, wet planets that reside within their habitable zones, which are only about one-fifth to 1/50th of the width of that for a G star. Particularly in light of the claimed detection of the planets with masses as small as 5.5 and 7.5 M(Earth) orbiting M stars, there seems no reason to exclude the possibility of terrestrial planets. Tidally locked synchronous rotation within the narrow habitable zone does not necessarily lead to atmospheric collapse, and active stellar flaring may not be as much of an evolutionarily disadvantageous factor as has previously been supposed. We conclude that M dwarf stars may indeed be viable hosts for planets on which the origin and evolution of life can occur. A number of planetary processes such as cessation of geothermal activity or thermal and nonthermal atmospheric loss processes may limit the duration of planetary habitability to periods far shorter than the extreme lifetime of the M dwarf star. Nevertheless, it makes sense to include M dwarf stars in programs that seek to find habitable worlds and evidence of life. This paper presents the summary conclusions of an interdisciplinary workshop (http://mstars.seti.org) sponsored by the NASA Astrobiology Institute and convened at the SETI Institute.     

基于USB的数据存储设备开发方案

介绍一个基于USB的数据存储设备开发方案,系统采用PH ILIPS公司的ISP1160芯片来实现USB主机控制器。首先介绍USB的特点,然后详细讨论方案各功能模块的实现方法,最后说明方案应用和系统性能指标。     

星间异步通信链路的误码率测试技术

误码率是星间链路通信系统中的一个重要指标。文章提出了适用于星间双向异步通信链路直传、转发模式的误码率测试方法,通过串口一网口转换方案实现了对多节点的星间通信链路进行数据传输误码率检测。设计了双向异步信道传输误码分析算法并利用软件实现,提供对星间链路多种码型、多种传输帧协议的误码率测试功能,能够给出双向异步信道传输误码的详细参数,分析星间双向异步通信链路的误码成因。     

基于粒子群优化核极限学习机的北斗超快速钟差预报

针对卫星钟差序列中非线性特性较为复杂和超快速钟差预报精度较低的问题,将核极限学习机算法引入到北斗超快速钟差预报中。首先,将极限学习机进行优化,引入粒子群优化算法来选择核极限学习机所需的核参数和正则化参数;然后,将优化后的方法应用到超快速钟差预报中,并给出了利用该方法进行超快速钟差预报的步骤;最后,在分析iGMAS提供的实测北斗超快速钟差数据的基础上,选用单天和多天数据进行短期预报。结果表明：在短期预报6h范围内,利用本文提供的优化方法解算得到的超快速钟差预报精度明显优于二次多项式模型和周期项模型,并且采用此方法得到的超快速钟差预报产品与iGMAS提供的超快速钟差预报产品(ISU-P)相比,GEO、IGSO和MEO卫星的预报精度分别提升了50.51%、46.98%、40.67%,其与最终精密钟差的符合程度显著 增强 。     

基于小卫星平台的超光谱成像ORASIS探讨

文章对国内外星载超光谱成像系统的应用状况进行了归纳．重点对其应用特点和关键技术进行了总结。在此基础上阐述了基于小卫星平台的超光谱成像系统的技术优势,探讨了利用小卫星姿轨机动灵活和可组成分离异构星座的特点,来实现星载超光谱系统对地实时成像以及解决海量数据处理和传输等关键问题的可行性。并着重对研制适应小卫星平台的集约型超过...     

试验箱风速对航天器部件常压低温热变形试验的影响分析

文章以航天器机械臂为研究对象,采用流-热-固耦合方法仿真分析了单一送风形式下,试验箱不同送风速度对机械臂常压低温热变形的影响,并进行了试验验证。分析发现:随着送风速度的增大,机械臂表面的温度场分布更均匀且温度值更接近于设定值,从而更有利于低温热变形试验的实施;但由于存在环境噪声,必须经过静置稳定后才可以进行变形测量。此分析结果可以用于指导航天器部件常压低温热变形试验更加精确、高效地实施。     

柔性空间飞行器的振动抑止控制

本文提出了一种带有柔性附件的卫星的振动主动抑止方法,给出了能抑止任意阶振动谐波的条件.作为举例,分析了太阳帆板的转动控制,在使帆板平稳旋转的同时,还使卫星姿态稳定无振.     

A permanently-acting NEA damage mitigation technique via the Yarkovsky effect

In the later stages of a combined mission of exploration and damage mitigation of a hazardous Near Earth Asteroid (NEA), sufficiently detailed tracking, orbit prediction, mass distribution, and physical properties data have been accumulated. It may be desirable to implement a “slow push” damage mitigation technique that is capable of altering the NEA orbit continuously and permanently. This possibility was suggested in a companion paper that outlined an archetypal exploration/mitigation mission to the NEA 99942 Apophis, which is achieved using a novel albedo change approach. The details and apparatus used in the albedo modification technique are described in the paper. We describe the design details and the constraints on particle size (to prevent electrostatic levitation and escape) and on the dispensing speed (to achieve the desired coverage zone and prevent particles from orbiting or escaping).     

皮卫星星箭分离动力学模拟及其灵敏度分析

皮卫星能源有限、姿控能力差等特点决定其对星箭分离初始姿态要求较高。在采用自主研发的皮卫星星箭分离机构的基础上,以多体动力学理论为基础,采用ADAMS软件建立了皮卫星及其星箭分离机构虚拟样机模型,分别就皮卫星质心偏离量、分离弹簧与舱门扭簧弹性系数对入轨初始姿态影响展开了分析。分析结果表明：质心偏心量对分离姿态影响最明显,分离弹簧与舱门扭簧弹性系数对其影响次之,合理配置分离弹簧与舱门扭簧弹性系数有利于卫星保持良好的姿态分离。在轨分离试验显示：分离时刻皮卫星滚动角速度、俯仰角速度、偏航角速度分别为-0.18（°）/s,-1.6（°）/s,0.95（°）/s,与在轨环境下仿真结果基本相符;入轨初始姿态能满足皮卫星的姿控要求,为其后续工作提供了保障。     

Methodology for Multiaircraft Minimum Noise Impact Landing Trajectories

The problem of optimizing landing trajectories with respect to noise impact index is addressed. In contrast with previous work, multilandings are considered. In order to make the problem tractable the trajectories are specified in functional form with certain parameters left free for selection by the optimization methods. Constraint of aircraft dynamic behavior, trajectory separation, pilot workload, passenger comfort, and maximum noise intensity all enter into the determination of what is an allowable trajectory. A version of the quasi-Newton iterative procedure is used to determine the optimum parameter values. The results show improvement in noise impact to the airport considered and the potential for even greater improvement at many airports.